Differential Rotation in Stars on the Upper Main Sequence

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Abstract
Models for slowly rotating stars on the upper main sequence are constructed without radiation pres- sure The well-known indeterminancy in the distribution of stellar angular momentum is removed by applying either of two supplementary boundary conditions which are due to the circumstance that radia- tive viscosity and the radiative transport of angular momentum are relatively large in the outer envelopes of luminous stars. For all the models, the angular velocity at the surface is smaller than the constant value in the rigidly rotating, convective core. One of the extra boundary conditions gives rise to a small equa- torial acceleration at the outer boundary, whereas the other requires a strong equatorial deceleration, the angular velocity at the equator in the latter case being as small as 6 percent of the central value. In the interior, surfaces of constant angular momentum per unit mass are approximately cylindrical, a circum- stance which favors the stability of these solutions

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